Measurements of the solar coronal magnetic field based on coronal seismology with propagating Alfvenic waves: forward modeling

TL;DR

This study uses forward modeling of MHD simulations to validate coronal seismology techniques for measuring the solar magnetic field via propagating Alfvenic waves, highlighting accuracy and potential error sources.

Contribution

It introduces a forward modeling approach to verify the reliability of coronal seismology in magnetic field measurements using propagating kink waves.

Findings

Seismology accurately infers magnetic field and plasma density.

Comparison confirms the method's reliability.

Identifies factors causing measurement errors.

Abstract

Recent observations have demonstrated the capability of mapping the solar coronal magnetic field using the technique of coronal seismology based on the ubiquitous propagating Alfvenic/kink waves through imaging spectroscopy. We established a magnetohydrodynamic (MHD) model of a gravitationally stratified open magnetic flux tube, exciting kink waves propagating upwards along the tube. Forward modeling was performed to synthesize the Fe XIII 1074.7 and 1079.8 nm spectral line profiles, which were then used to determine the wave phase speed, plasma density, and magnetic field with seismology method. A comparison between the seismologically inferred results and the corresponding input values verifies the reliability of the seismology method. In addition, we also identified some factors that could lead to errors during magnetic field measurements. Our results may serve as a valuable reference for current and future coronal magnetic field measurements based on observations of propagating kink waves.